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Binary neutron star mergers probe the dense-matter equation of state (EoS)across a wide range of densities and temperatures, from the cold conditions ofthe inspiral to the high-temperature matter of the massive neutron starremnant. In this paper, we explore the sensitivity of neutron star mergers touncertainties in the finite-temperature part of the EoS with a series of mergersimulations performed in full general relativity. We expand on our previouswork to explore the interplay between the thermal prescription and thestiffness of the zero-temperature EoS, which determines the compactness of theinitial neutron stars. Using a phenomenological model of the particle effectivemass, $M^*$, to calculate the finite-temperature part of the EoS, we performmerger simulations for a range of thermal prescriptions, together with two coldEoSs that predict either compact or large-radius initial neutron stars. Wereport on how the choice of $M^*$-parameters influences the thermal propertiesof the post-merger remnant, and how this varies for stars with differentinitial stellar compactness. We characterize the post-merger gravitational wavesignals, and find differences in the peak frequencies of up to 190 Hz dependingon the choice of $M^*$-parameters. Finally, we find that the total dynamicalejecta is in general only weakly sensitive to the thermal prescription, butthat a particular combination of $M^*$-parameters, together with a soft coldEoS, can lead to significant enhancements in the ejecta.

Influence of stellar compactness on finite-temperature effects in neutron star merger simulations